期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 497, 期 2, 页码 1563-1570出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa2018
关键词
black hole physics; gravitational waves; stars: black holes; stars: kinematics and dynamics; stars: neutron; galaxy: open clusters and associations: general
资金
- European Research Council [770017]
- European Union's Horizon 2020 research and innovation programme under the Marie-Sklodowska-Curie grant [794393]
- Universita degli Studi dell'Insubria through a Cycle 33rd PhD grant
- European Research Council (ERC) [770017] Funding Source: European Research Council (ERC)
- Marie Curie Actions (MSCA) [794393] Funding Source: Marie Curie Actions (MSCA)
Young star clusters are likely the most common birthplace of massive stars across cosmic time and influence the formation of compact binaries in several ways. Here, we simulate the formation of black hole-neutron star binaries (BHNSs) in young star clusters, by means of the binary population synthesis code MOBSE interfaced with the N-body code NBODY6++GPU. BHNSs formed in young star clusters (dynamical BHNSs) are significantly more massive than BHNSs formed from isolated binaries (isolated BHNSs): similar to 40 per cent of the dynamical BHNS mergers have a total mass of >15M(circle dot), while only similar to 0.01 per cent of the isolated BHNS mergers have mass in excess of this value. Hence, our models strongly support a dynamical formation scenario for GW190814, given its total mass of similar to 26 M-circle dot, if this event is a BHNS merger. All our dynamical BHNSs are ejected from their parent star cluster before they reach coalescence. Thus, a significant fraction of BHNS mergers occurring in the field might have originated in a young star cluster. The mass spectrum of BHNS mergers from gravitational-wave detections will provide a clue to differentiate between dynamical and isolated formation of BHNSs.
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